Introduction Many astronomers study the brightest stars whose distribution is likely a great circle or belt. By the eighteenth century, William Herschel used star-gauging to study our Milky Way system and noticed the OB stars were not distributed uniformly (e.g., Whitney, 1971; Herschel, 1912). Gould (1879) found out the special distribution of the OB stars that were aligned along a great circle, which might not belong to the galactic plane and inclined about 20 degree. Since then, it is known as the Gould Belt. The investigation of the Gould Belt In the beginning, the Gould Belt was discovered by eyes, but many researches have studied the Gould Belt to check its existence in different investigating methods. The OB stars were observed easily and were made use of investigating the Gould Belt much frequently. The stellar motion of the O – B5 stars in the solar neighborhood has been discussed by Blaauw since 1956. Because the OB associations tend to expand, the expansion model is proposed at the time to estimate the age of the Gould Belt and the calculated age is 50 Myr (Blaauw, 1956). From the O – B5 stars of HD catalogue with absolute magnitude less than 6.5, investigation showed two kinds of the age of the selected OB stars. Age of B type stars might be about 90 Myr, which was different from considering OB association alone, if the stars were assumed to be an expansion model (Lesh, 1968). In fact, the age of the Gould Belt is in a range between 30 Myr and 90 Myr according to the different studying ways. If the Gould Belt is investigated about the stars occupying in the Gould Belt, the age will almost be 30 Myr ~ 50 Myr (Blaauw, 1956; Palouš, 1985; Westin, 1985; Comerón et al., 1994). Moreover, the age will be 30 ~ 90 Myr (Olano, 1982; Westin, 1985; Frogel & Stothers, 1977; Comerón & Torra, 1990; Pöpel et al., 1994; Lesh, 1968) when counted by the expansive rate. In 1973, the Gould Belt were thought to be with relation to the HI structure “feature A” by Lindblad and the research continued looking for the relation between the neutral gas and the Gould Belt. The Gould Belt was known to locate on the similar region of the “feature A” (Lindblad et al., 1973, 1997, 2000) and was discovered that the region contained stars, dust, HI, and the molecular clouds (e.g. Pöppel & Olano, 1982; Sandqvist, Tomboulides, Lindblad, 1988; Taylor & Dickman, 1987). In addition to the components of the Gould Belt, some researchers studied its kinematics and the interrelationship between galactic plane and the Gould Belt. When (X, Y, Z) and (U, V, W) of 280 OB stars are calculated, the horizontal velocity gradient ∂U/∂X is about 40 km/sec/kpc and infects these stars should be from Cassiopeia – Taurus and Scorpio – Centaurus groups (Eggen, 1961, 1975). Besides, Comerón (1999) provided that the motion of the Gould Belt still has a vertical component of the velocity. The kinematical properties of the Gould Belt affect not only the velocity gradient but also the stars in the solar neighborhood. When the kinematics of the stars in the solar neighborhood is discussed, the kinematics of the stars with R > 600 pc is determined by the galactic differential rotation and that with R ≦ 600 pc is lead by the Gould Belt (Torra et al., 2000). The character could be known by calculating the Oort’s constants, too (e.g. Uemura et al., 2000; Mignard, 2000; Dehnen & Binney, 1998; Tsioumis & Frick, 1979; Comerón, 1999; Olano, 1982). Furthermore, some researches didn’t study the early type stars but late type ones. The F-M stars, which exhibit active x-ray, were observed in x-ray by Guillout et al. (1998). The research shows that the Gould Belt can be discussed with late type stars from different x-ray energy. Besides, the investigation proposed that the Gould Bet could be a ring disk with small inner radius rather than a belt. The distribution of the Gould Belt drawn by Guillout et al. (1998) is Fig 1. Fig 1: The diagram of the Gould Belt projected on the XY-plane is from Guillout et al. (1998) according to the observation. The edge is defined by molecular clouds and the dash line is about 500 pc from the sun. The mark is the position of the sun, which doesn’t locate at the center of the Gould Belt. The semi-major is 500 pc in the direction of l = 15°/195°, and the semi-minor is about 340 pc in the direction of l = 105°/285° The distribution of the Gould Belt Some results of inclining angle with respect to the Galaxy and direction of the semi-major axis of Gould belt are listed on table 1 and table 2. The inclining angle with respect to the galactic plane is pretty different due to the different observing method. According to the radio observation, the inclining angle of the gas in the Gould Belt region is larger than that of the stars belonging to the Gould Belt (Strauss et al., 1979). The shape of the Gould Belt is not a circle or a ring due to the effect of galactic differential rotation, and the velocities of these stars belonging to the Gould Belt have changed their directions (e.g. Moreno et al., 1999; Torra et al., 1994). When the Gould Belt is projected in the sky, it seems to wind around the Milky Way. On the other hand, the projection of the Gould Belt on the XZ, or YZ plane shows an oblique belt or line and the length of the projective region won’t be the same in the two planes. Table 1: The inclination and deflection of the Gould Belt l , d(*) semi-major semi-minor notes l = 131°, d = 166 pc 364 pc 211 pc Olano (1982) l = 150°, d = 140 pc 326 pc 157 pc Lindblad et al. (1973) l = 135°, --- --- Westin (1985) l = 127°, --- --- Lindblad (2000) *: l and d are direction and distance of the center of Gould belt from the sun, respectively. Table 2: The parameters of the Gould Belt φ°(*) l°(+) The way for studying notes The distribution of the complex O – B5, Frogel & Stothers ~ 18 25 luminous supergiants, clusters and (1974) associations The photometric and motion of 500 early 22 --- Eggen (1975) type stars brighter than Mv = -1 The positions and velocities of the selected 19 --- Poluš (1985) younger A type and B type stars from CDS 19 (age < 2×107) The spatial and kinematics of the O – A0 --- Westin (1985) 14 (age = 3 ~6×107) stars with age younger than 6×107 years CO emission survey of 622 molecular 12.5 --- Taylor et al. (1987) clouds in the solar neighborhood Selecting 2483 stars with V < 7.5 discussed Comeron et al. 22.3 --- the characteristics and origin (1994) Analyzing 90000 A, F, G type dwarfs at an Fresnueau et al. 20 --- altitude over the Galactic plane lower than (1996) 300 pc The X-ray luminosity of F – M type stars of the RASS – Tycho. (Data with Lx = 1029.5 ~ Guillout et al. 25 20 1031 erg/sec which is commensurate with the (1998) age of Gould Belt are discussed.) The kinematical model and distribution of 6922 O- and B- type stars from Hipparcos 16 ~ 22 --- Torra et al. (2000) Internal Proposal INC4060 completed with all the O and B survey stars * φ ：Direction of the semi-major axis + l ：Inclining angle with respect to the Galaxy The origin of the Gould Belt The origin of the Gould Belt is still a puzzle. The most reasonable explanations are single explosive event like super novae explosion (e.g. Blaauw, 1956, 1991; Lesh, 1968; Olano, 1982; Sandqvist et al., 1988; Torra et al., 2000; Lindblad, 1973, 2000), the impact of a large high velocity cloud (e.g. Comerón & Torra, 1992,1994), and the effect of spiral density waves (e.g. Lindblad et al., 1973). Blaauw (1956) pointed out that the dynamics of the Gould Belt might be contained a property about expansion. In addition, it may be also has a rotational property with a pretty large initial angular momentum and velocity dispersion, which make the Gould Belt gravitationally unbound and continue expanding (Lindblad et al., 1968, 1997). To explain the expansion and rotation model, the Gould Belt could be assumed as forming from a giant molecular cloud with a rotation axis (e.g. Fresneau et al,.1996; Lindblad, 1997; Comeron, 1999). When a shock wave passes this giant molecular cloud, young stars emerge in the region where is the Gould Belt (Fresneau et al., 1996). Stars in the region would keep some properties of the shock wave due to the explosion, and they look like moving outward. On the other hand, the rotation axis is not perpendicular to our galactic plane, so Comerón (1999) proposed that it would be high velocity clouds give rise to the Gould Belt forming. When a high velocity cloud collides on the galactic disk, the shock would advance the shocked gas. The shock front breaking down the equilibrium is the main reason of the star formation in the shocked region. The model can explain the expansion of the Gould Belt reasonably, too. No matter what the origin is, it can make a shock wave concentrate the interstellar medium then cause the formation of molecular clouds and stars by gravitational instabilities (e.g. Palouš, 1994; Mc Cray, 1987; Elmegreen, 1989,1992). Furthermore, the Gould Belt still exists without damping in present by the balance of the radiative force and the ambient interstellar pressure (Elmegreen & Chiang, 1982; Moreno et al., 1999; Franco et al., 1991).